Measurements of cosmic-ray secondary nuclei at high energies with the first flight of the CREAM balloon-borne experiment

By H. Ahn, P. Allison, M. G. Bagliesi, J. Beatty, G. Bigongiari, P. Boyle, T. Brandt, J. Childers, N. Conklin, S. Coutu and 61 more. 2008

149 citations recorded by the source corpus.

Abstract We present new measurements of heavy cosmic-ray nuclei at high energies performed during the first flight of the balloon-borne cosmic-ray experiment Cosmic-Ray Energetics and Mass (CREAM). This instrument uses multiple charge detectors and a transition radiation detector to provide the first high accuracy measurements of the relative abundances of elements from boron to oxygen up to energies around 1 TeV/n. The data agree with previous measurements at lower energies and show a relatively steep decline (∼ E −0.6 to E −0.5 ) at high energies. They further show the source abundance of nitrogen relative to oxygen is ∼10% in the TeV/n region.

Subfields: Nuclear and High Energy Physics, Pulmonary and Respiratory Medicine

View Paper: https://www.semanticscholar.org/paper/91140606821427f344ef6525f38a0bb628a627d0

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In Nuclear and High Energy Physics

Citations in the corpus

ENERGY SPECTRA OF COSMIC-RAY NUCLEI AT HIGH ENERGIES (2009, methodology): “Unlike the primary heavy nuclei, nitrogen is mostly produced by spallation in the inter- stellar medium, but it also has a primary contribution of order 10%, as recently measured by CREAM-I (Ahn et al. 2008).”
A database of charged cosmic rays (2013, unknown): “– Balloon (1982/10): Garcia-Munoz et al. (1986) – Balloon (1984/09): Garcia-Munoz et al. (1986) – Balloon (1987/08): Evenson et al. (1995) – Balloon (1990/08): Evenson et al. (1995) – Balloon (1992/08): Evenson et al. (1995) – Balloon (1994/08): Evenson et al. (1995) – Balloon (1969/04+1970/11): Sil”
A Markov Chain Monte Carlo technique to sample transport and source parameters of Galactic cosmic rays - II. Results for the diffusion model combining B/C and radioactive nuclei (2010, methodology): “…et al. 1987), the Voyager 1&2 (Lukasiak et al. 1999), and the ACE-CRIS (de Nolfo et al. 2006) spacecrafts; ii) intermediate energies acquired by HEA0-3 data (Engelmann et al. 1990); and iii) higher energy data from Spacelab (Swordy et al. 1990) and the published CREAM data (Ahn et al. 2008).”
GIANT GAMMA-RAY BUBBLES FROM FERMI-LAT: ACTIVE GALACTIC NUCLEUS ACTIVITY OR BIPOLAR GALACTIC WIND? (2010, methodology): “We use the estimated diffusion constant from GALPROP, K = 5.3×1028 cm2/s at a reference rigidity of 4 GV, and take the diffusion coefficient index to be δ = 0.43 following the results of Ahn et al. (2008).”
DISCREPANT HARDENING OBSERVED IN COSMIC-RAY ELEMENTAL SPECTRA (2010, methodology): “The TRD analysis and measurement of the secondary-to-primary (e.g., B/C) ratio have been reported elsewhere (Ahn et al. 2008).”
Diffusive propagation of cosmic rays from supernova remnants in the Galaxy. II: anisotropy (2011, background): “Unfortunately at the present time the error bars on this quantity are still large enough to allow for ambiguity in the best fit value (see for instance [28]).”
COSMIC-RAY PROTON AND HELIUM SPECTRA FROM THE FIRST CREAM FLIGHT (2011, methodology): “Results from the CREAM experiment such as B/C ratio and heavy elemental spectra are discussed in elsewhere (Ahn et al. 2008, 2009a, 2010).”
CONSTRAINTS ON COSMIC-RAY PROPAGATION MODELS FROM A GLOBAL BAYESIAN ANALYSIS (2010, methodology): “At higher energies, from 30 GeV/nucleon – 1 TeV/nucleon, we use ATIC-2 (Panov et al. 2008) and CREAM-1 data (Ahn et al. 2008).”